Besides quantifying the relative contribution of SNIa and SNcc to the enrichment of the IGrM, elemental abundance ratios may also reveal the nature of the so far unexplained abundance drops that are sometimes observed (see §REF ) in the very inner centers of groups and clusters.
Under the assumption that these abundance drops have an astrophysical origin, an interesting scenario proposed by [1]}, [2]} considers that IGrM-phase metals may deplete into dust and then become invisible to the X-ray window. As a second step, AGN jets and buoyantly rising bubbles may contribute to move this dust mass away, before eventually re-heating it to the X-ray phase outside of the very core. If true, an interesting corollary of this scenario concerns the Ne and Ar abundance. As these two elements are noble gases, they can not be incorporated into dust, hence they should not exhibit any central decrease. Although a few authors have investigated this issue [3]}, [4]}, [5]}, no real consensus is established yet given the sensitivity of the measurements to systematic effects. Ar and Ne lines should be easily measurable with future micro-calorimeters (Sect. ). Provided that atomic codes continue to converge (Sect. REF ) in the years to come, Athena (and possibly XRISM for very nearby systems) will provide a definitive answer to this question.
